Physics
Scientific paper
Mar 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004pfte.confe..10k&link_type=abstract
Presented at the KITP Conference: Planet Formation: Terrestrial and Extra Solar, Mar 15, 2004, Kavli Institute for Theoretical P
Physics
Scientific paper
The time evolution of a system of two protoplanetsstill embedded in a protoplanetary disk has been studiedviscous hydrodynamical simulations.Resonant capture of the planets is seen, wherethe order of the resonance depends on the initial spatial separation of theplanets, and the properties of the disk and the planets.Resonant capture leads to a rise in the eccentricity and to analignment of the spatial orientation of orbits.The numerical results are compared with the observed planetarysystems in mean motion resonance (GJ~876, HD~82943, and 55~Cnc).We find that the forcing together of two planets by their parent diskproduces resonant configurations similar to those observed,but that eccentricity damping greater than that obtainedin our hydrodynamic simulations is required to match theGJ~876 observations.
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